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  • Humans
  • Lunar and Planetary Science and Exploration
  • 1960-1964  (5)
  • 1
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    Fossil Glasses Produced by Impact of Meteorites, Asteroids and Possibly Comets with the Planet Earth (1962)
    In:  CASI
    Details
    Publication Date: 2019-08-14
    Description: In recent times one of the most intriguing mysteries of geology bas been the occurrence of aerodynamically-shaped glasses on five continents of the earth. These glasses under discussion are obviously not of fulgurite origin. Recent research indicates that these glasses known as tektites are ~he result of meteorite, asteroid, or possibly comet impact. Impact glasses, in general, differ from volcanic glasses in that they are lower in water content, have lower gallium and germanium contents, and are not necessarily in magmatically unstable continental areas.
    Keywords: Lunar and Planetary Science and Exploration
    Type: HQ-E-DAA-TN70721 , International Congress on Glass; Jul 08, 1962 - Jul 12, 1962; Washington, DC; United States
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 2
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    The Atmosphere and Haze of Mars (1960)
    In:  CASI
    Details
    Publication Date: 2019-08-14
    Description: The 'blue haze' is an absorbing smoke, dark as soot in reflection, red in transmission. Its currently accepted explanation by pure scattering (omnidirectional or forward) is untenable, as it would either increase the surface brightness of fall to obscure the surface details. The limb darkening of Mars is mainly the results of absorption by the smoke. The opacity of the Martian atmosphere increases from the red toward the violet. The extinction by the Martian atmosphere is greater than that by the terrestrial at all wavelengths, but only about 20 per cent of the Martian extinction is due to scattering. Dollfus' polarimeteric estimate, corrected for self-absorption, corresponds to a martian atmospheric pressure of 87 mm Hg. The photochemical breakup of carbon dioxide and the escape of oxygen must lead to considerable concentrations of carbon monoxide in the martian atmosphere.
    Keywords: Lunar and Planetary Science and Exploration
    Type: 41st Annual Meetins, Sessions on Planetary Sciences, American Geophysical Union; Apr 27, 1960 - Apr 30, 1960; Washington, DC; United States|Journal of Geophysical Research; 65; 10; 3057-3063
    Format: text
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    NASA TECHNICAL REPORTS
  • 3
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    Objectives of the Mariner Venus Microwave Radiometer Experiment (1961)
    In:  CASI
    Details
    Publication Date: 2019-08-14
    Description: At present, there are several models involving the surface, atmosphere (and ionosphere), and cloud conditions of the planet Venus which attempt to account for the observed high brightness temperature of 600 degrees Kelvin in the microwave temperature region. None of these models can be definitely accepted or rejected on the basis of presently available data, and it is the goal of the microwave radiometer experiment planned for the Mariner Venus mission to determine which of the proposed models most nearly approximates Venusian conditions. The disc of the planet will be scanned at 4 wavelengths - 4, 8, 13.5 and 19 millimeters - to measure the temperature distribution across the planet. Measurement accuracy is expected to be to within 2 percent. In addition to the study of gross thermal characteristics of surface and atmosphere (or ionosphere), some information regarding the fine-scale thermal variations will be obtained. Since Venus appears to be continuously covered by clouds, it is obvious that only in the microwave region can one be sure of penetrating clear to the solid surface. Because of the absorbing characteristics of the Earth's atmosphere, and because of the relatively poor resolution obtainable in this region of the spectrum, one is forced to utilize the platform afforded by a planetary flyby or orbiter in order to conduct a reliable high resolution study of the planet. To do so from Earth (neglecting terrestrial atmospheric attenuation ) would require colossal radio telescopes.
    Keywords: Lunar and Planetary Science and Exploration
    Type: JPL-TR-32-156
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  • 4
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    Survey of the Physical and Environmental Parameters of the Moon (1963)
    In:  CASI
    Details
    Publication Date: 2019-08-17
    Description: This document presents, in summary, a compilation of the physical and environmental parameters of the moon. A determined attempt has been made to be objective at all times. Many of the physical sciences are presented in sufficient depth to adequately identify the basic information available. It is expected that the appropriate references will be consulted when additional detail is required. It is obvious both from the text and the reference material that divergent opinions prevail and uncertainties exist in almost every phase of lunar science; e.g., the existence of the lunar bulge, the thickness of the dust layer, etc. No pretense is made to resolve these differences, but by bringing together many references, it is hoped that some contribution will be made in lunar science. The subject index will be of particular value since it relates the reference section by subject. A glossary of terms used throughout the text is also provided.
    Keywords: Lunar and Planetary Science and Exploration
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  • 5
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    Lunar Brightness Variations with Phase at 4.3-MM Wave Length (1961)
    In:  Other Sources
    Details
    Publication Date: 2019-08-26
    Description: The lunar radio observations and interpretations of Piddington and Minnett (1949) and Gibson (1958) show that the lunar brightness variation with phase at millimeter wave lengths can be used to determine the physical properties of the lunar surface. They found that the millimeter-wave brightness lagged the optical phase, and their interpretation was that the millimeter radiation originates below a surface layer that is a very good thermal insulator. The thickness of this layer could not be determined from observations at one frequency. Observations at different frequencies give different results because of the wave-length dependence of the radio absorption by the surface material. The attenuation in the material increases with decreasing wave length, and therefore it is possible, in principle, to determine surface layer thickness from radio observations at several wave lengths. For this reason, observations of lunar radiation were started at the Naval Research Laboratory at a wave length of 4.3 mm. This is half the wave length used by Gibson (1958) in his earlier studies. The radio telescope used for these observations has been described in detail in a previous publication (Coates 1958). The antenna is a parabolic reflector 10 feet in diameter, and it has a beam width of 6.7 minutes of arc at the wave length of 4.3 mm. This is about one-fifth the diameter of the moon. The receiver was a Dicke-type radiometer.
    Keywords: Lunar and Planetary Science and Exploration
    Type: The Astrophysical Journal; 133; 2; 723-725
    Format: text
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